skip to main content
Idioma:
Tipo de recurso Mostra resultados com: Mostra resultados com: Índice

Numerical simulation of satellite-ring interactions: Resonances and satellite-ring torques

Brophy, Thomas G. ; Esposito, Larry W. ; Stewart, Glen R. ; Rosen, Paul A.

Icarus (New York, N.Y. 1962), 1992-12, Vol.100 (2), p.412-433 [Periódico revisado por pares]

Legacy CDMS: Elsevier Inc

Texto completo disponível

Citações Citado por
  • Título:
    Numerical simulation of satellite-ring interactions: Resonances and satellite-ring torques
  • Autor: Brophy, Thomas G. ; Esposito, Larry W. ; Stewart, Glen R. ; Rosen, Paul A.
  • Assuntos: Astronomy ; Astronomy & Astrophysics ; Earth, ocean, space ; Exact sciences and technology ; General, solar nebula, and cosmogony ; Lunar And Planetary Exploration ; Physical Sciences ; Science & Technology ; Solar system
  • É parte de: Icarus (New York, N.Y. 1962), 1992-12, Vol.100 (2), p.412-433
  • Notas: CDMS
    Legacy CDMS
    ObjectType-Article-2
    SourceType-Scholarly Journals-1
    ObjectType-Feature-1
    content type line 23
  • Descrição: A kinetic equation is solved numerically for a flattened planetary ring which is perturbed gravitationally by a near-by satellite. The Krook kinetic equation for planetary rings is solved in two spatial dimensions, and in time, with interparticle collisions, with satellite forcing, and without self-gravity. The phase-space fluid numerical method is extended to two-dimensional systems by ignoring negligible high-order velocity moments. In simulations of satellite induced wakes, we verify the role of local shear reversal and angular momentum flux decrease as described by Borderies et al. (1983, Icarus 55, 124–132). A new result is that the amplitude of wakes is limited by purely kinematic effects, even in the absence of collisions. The results of a simulation of an inner Lindblad resonance location, as the distribution approaches steady-state, are presented in detail. The surface mass density, pressure tensor components, and mean velocities are calculated during the simulation. The detailed mechanisms of local torque balance and forced eccentricity “damping” at resonance are illuminated. The angular momentum flux perturbations play the critical role of balancing the satellite torque on the surface mass density asymmetry. The eccentricities very close to resonance are limited by collisional phase mixing. The resulting near steady-state distribution feels a net radially integrated torque of essentially zero from the satellite to the first-order accuracy intended by the method, though there are large negative and positive torques on the regions just inside of and outside of the exact resonance. We show that previous analytic calculations of the torque (which show nonzero net torque) were the result of small second-order deviations of the surface density on top of the large first-order structure which our simulations reproduce, while there are second-order effects not accounted for in those calculations. Our simulations do not show an increase of the velocity dispersion in the resonance zone, so that energy conservation considerations do not require a net torque due to conservation of the Jacobi constant of the planar restricted three-body problem. We therefore argue that simulations or calculations which include all second-order effects are needed in order to determine the torques which will actually occur in rings.
  • Editor: Legacy CDMS: Elsevier Inc
  • Idioma: Inglês
Links
Voltar para lista de resultados

  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

Buscando em bases de dados remotas. Favor aguardar.